Turbulence, intermittency and cross-scale energy transfer in an interplanetary coronal mass ejection

TL;DR

This study analyzes MHD turbulence properties within an interplanetary coronal mass ejection using spacecraft data, confirming turbulence development and high energy transfer rates, especially in the ICME sheath region.

Contribution

It provides a detailed characterization of turbulence and energy transfer in an ICME, validating the third-order law and highlighting enhanced intermittency and energy injection.

Findings

Turbulence within the ICME shows developed spectral and flatness scaling.

The third-order moment scaling law is validated in all sub-regions.

High energy transfer rates are observed in the ICME sheath, indicating intense energy injection.

Abstract

Solar wind measurements carried out by NASA's Wind spacecraft before, during and after the passing of an interplanetary coronal mass ejection (ICME) detected on 12-14 September 2014 have been used in order to examine several properties of magnetohydrodynamic (MHD) turbulence. Spectral indices and flatness scaling exponents of magnetic field, velocity and proton density measurements were obtained, and provided a standard description of the characteristics of turbulence within different sub-regions of the ICME and its surroundings. This analysis was followed by the validation of the third-order moment scaling law for isotropic, incompressible MHD turbulence in the same sub-regions, which confirmed the fully developed nature of turbulence in the ICME plasma. The energy transfer rate was also estimated in each ICME sub-region and in the surrounding solar wind. An exceptionally high value was found within the ICME sheath, accompanied by enhanced intermittency, possibly related to the powerful energy injection associated with the arrival of the ICME.